The data were processed with the usual LoTSS pipelineThe LoTSS pipeline can be found at https://github.com/mhardcastle/ddf-pipeline [1]}, [2]} which is described in [3]}. We then performed an additional round of self-calibration in the direction of WX UMa with a procedure described in [4]} and also employed in [5]}.
After calibration, the measurement set was further processed to make source extraction easier for producing light curves and spectra. WX UMa was removed from the mask image which was then used to produce a model file using WSClean. WX UMa was also removed from these model images so that it would not be removed during the subtraction of other sources. The subtracted model image was then used with WSClean again to predict visibilities which were recorded in a new modelled data column in the measurement set. The modelled data was subtracted from the real data column and recorded in a new column - this served to remove all other bright sources from the region besides WX UMa. Finally, DPPP was used to phaseshift the measurement sets to be centred on WX UMa, using the subtracted data as the new real data.
